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| Paper: |
Star Formation and Cosmic Massive Black Hole Formation, A Universal Process Organised by Angular Momenta |
| Volume: |
323, Star Formation in the Interstellar Medium: In Honor of David Hollenbach, Chris McKee, and Frank Shu |
| Page: |
261 |
| Authors: |
Colgate, S.A. |
| Abstract: |
It is suggested that star formation is organized following the same principles as we have applied in a recent explanation of galaxy and massive black hole formation. In this scenario angular momentum is randomly distributed by tidal torquing among condensations, Lyman-α clouds or cores for star formation during the initial non-linear phase of collapse. This angular momentum is characterized by the parameter, λ, the ratio of the angular momentum of the cloud to that of a Keplerian orbit with the same central mass and radius. This parameter is calculated in very many simulations of structure formation of the universe as well as core formation and appears to be universal and independent of any scale. The specific angular momentum during the collapse of every cloud is locally conserved and universally produces a near flat rotation curve M<R ∝ R. The initiation of the first transport of angular momentum within such a disk occurs at a given critical thickness, Σcrit ≈ 300 g/cm2 for galaxies and Σcrit ≈ 2000 g/cm2 for stellar disks where the Rossby Vortex Instability (RVI) can grow. The mass inside the radius of this condition collapses either to a massive galactic black hole, 108 Solar masses, (∼ 10-3 of the galactic disk mass) or 1 Solar mass (∼ 0.03 of the core or of the protostellar disk mass). The inviscid collapse of a protosteller core with the same average λ ≈ 0.05 leads to the formation of a flat rotation curve (protostellar) disk of mass Mdsk ∼ 30 Solar masses of radius Rdsk ≈ 1100 AU or 5.4 × 10-3 pc. In such a disk Σ ∝ 1/R and reaches the RVI condition at Rcrit ≈ 40 AU where M<R ≈ 1 Solar mass. |
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